液体火箭发动机诱导轮空化热力学效应研究

为了研究空化热力学效应,以模型诱导轮为研究对象,改变流量、水温等条件,对其内部空化流动进行了可视化实验研究,完整记录了从空化初生至性能断裂点各工况的空化区形态。结果表明:温度对诱导轮无空化水力性能没有显著影响,但是高温下诱导轮的空化性能断裂点被显著延后,体现了热力学效应的影响。对比不同温度下的空化区形态,发现热力学效应的强弱与流动工况密切相关,在小空化数下体现得更为显著。同时引入一种半经验的理论模型预测热效应对空化性能的影响,小流量(Φ=0.071)下预测结果与实验结果平均偏差为5.5%,大流量(Φ=0.088)下平均偏差为10.8%,验证了模型在本文应用条件下的可靠性。     

垂直/短矩起降飞机机翼内埋式风扇布局气动特性分析

以垂直/短距起降飞机过渡飞行状态为背景,针对机翼内埋式风扇布局的自由来流/风扇喷流混合型流动,基于结构/非结构混合网格使用CFD方法进行了非定常数值模拟和分析.首先使用滑移网格技术对NASA涵道螺旋桨进行算例验证,其时均计算结果与实验值的误差为5.3%,证明了计算方法的可靠性和准确性,然后数值模拟了机翼内埋式风扇布局在不同迎角下的气动性能.结果表明:风扇喷流在机翼上产生了特有的“抽吸”和“堵塞”效应,引起了机翼总升阻力的显著增加,升力最大增量达到干净机翼升力的2.6倍,阻力最大增量为干净机翼阻力的3.2倍,混合流场在机翼后缘引起了升力损失并卷起对涡.      

基于拟动力学的航空发动机主轴球轴承热弹流润滑分析

以航空发动机主轴球轴承高速高温重载典型工况为算例,基于轴承拟动力学分析,得到滚动体与套圈之间的微接触区运动和受力状态,分别用Hamrock-Dowson(H-D)拟合公式和翟文杰热修正公式计算了最小膜厚(MFT),同时结合热弹流润滑分析得到最小膜厚分布,对比了试验测试、H-D拟合、翟文杰热修正和热弹流润滑分析4种算法的最小膜厚,并根据膜厚比判定了轴承的弹流润滑状态.结果表明:H-D拟合和翟文杰热修正最小膜厚与试验测试结果相差较远,热弹流润滑分析结果与试验数据吻合性较好,误差10%以内;探讨了不同工况下的轴承弹流润滑性能.结果表明:存在径向载荷时,润滑膜整体压力增大,膜厚减小;随着转速增大,压力减小,膜厚增大,但是增大的趋势减缓.      

叶尖泄漏流和引射效应对跨声速串列转子失速机制的影响

为探究跨声速串列转子的失速机制,利用数值模拟的手段对不同间隙情况的某跨声速串列转子的叶尖流场进行分析.研究发现:前排二次泄漏区会对失速产生重要影响;叶尖泄漏流和引射效应是前排二次泄漏区流场结构的决定因素,而间隙大小直接影响着两者的强弱.当前排大间隙时,叶尖泄漏流强,是前排二次泄漏区流场的主导因素,这时失速首先发生在前排;当前排间隙减小时,引射效应增强,并逐渐成为主导因素,这时前排二次泄漏区的堵塞情况得到改善,失速区域转移到后排.改变前排间隙对该跨声速转子的性能有更显著的影响,当前排为最先失速排时,改变后排间隙对串列转子性能没有显著影响.      

OSIRIS-REx: Sample Return from Asteroid (101955) Bennu

In May of 2011, NASA selected the Origins, Spectral Interpretation, Resource Identification, and Security–Regolith Explorer (OSIRIS-REx) asteroid sample return mission as the third mission in the New Frontiers program. The other two New Frontiers missions are New Horizons, which explored Pluto during a flyby in July 2015 and is on its way for a flyby of Kuiper Belt object 2014 MU69 on January 1, 2019, and Juno, an orbiting mission that is studying the origin, evolution, and internal structure of Jupiter. The spacecraft departed for near-Earth asteroid (101955) Bennu aboard an United Launch Alliance Atlas V 411 evolved expendable launch vehicle at 7:05 p.m. EDT on September 8, 2016, on a seven-year journey to return samples from Bennu. The spacecraft is on an outbound-cruise trajectory that will result in a rendezvous with Bennu in November 2018. The science instruments on the spacecraft will survey Bennu to measure its physical, geological, and chemical properties, and the team will use these data to select a site on the surface to collect at least 60 g of asteroid regolith. The team will also analyze the remote-sensing data to perform a detailed study of the sample site for context, assess Bennu’s resource potential, refine estimates of its impact probability with Earth, and provide ground-truth data for the extensive astronomical data set collected on this asteroid. The spacecraft will leave Bennu in 2021 and return the sample to the Utah Test and Training Range (UTTR) on September 24, 2023.

     

Imaging Plasma Density Structures in the Soft X-Rays Generated by Solar Wind Charge Exchange with Neutrals

Both heliophysics and planetary physics seek to understand the complex nature of the solar wind’s interaction with solar system obstacles like Earth’s magnetosphere, the ionospheres of Venus and Mars, and comets. Studies with this objective are frequently conducted with the help of single or multipoint in situ electromagnetic field and particle observations, guided by the predictions of both local and global numerical simulations, and placed in context by observations from far and extreme ultraviolet (FUV, EUV), hard X-ray, and energetic neutral atom imagers (ENA). Each proposed interaction mechanism (e.g., steady or transient magnetic reconnection, local or global magnetic reconnection, ion pick-up, or the Kelvin-Helmholtz instability) generates diagnostic plasma density structures. The significance of each mechanism to the overall interaction (as measured in terms of atmospheric/ionospheric loss at comets, Venus, and Mars or global magnetospheric/ionospheric convection at Earth) remains to be determined but can be evaluated on the basis of how often the density signatures that it generates are observed as a function of solar wind conditions. This paper reviews efforts to image the diagnostic plasma density structures in the soft (low energy, 0.1–2.0 keV) X-rays produced when high charge state solar wind ions exchange electrons with the exospheric neutrals surrounding solar system obstacles.The introduction notes that theory, local, and global simulations predict the characteristics of plasma boundaries such the bow shock and magnetopause (including location, density gradient, and motion) and regions such as the magnetosheath (including density and width) as a function of location, solar wind conditions, and the particular mechanism operating. In situ measurements confirm the existence of time- and spatial-dependent plasma density structures like the bow shock, magnetosheath, and magnetopause/ionopause at Venus, Mars, comets, and the Earth. However, in situ measurements rarely suffice to determine the global extent of these density structures or their global variation as a function of solar wind conditions, except in the form of empirical studies based on observations from many different times and solar wind conditions. Remote sensing observations provide global information about auroral ovals (FUV and hard X-ray), the terrestrial plasmasphere (EUV), and the terrestrial ring current (ENA). ENA instruments with low energy thresholds (\(\sim1~\mbox{keV}\)) have recently been used to obtain important information concerning the magnetosheaths of Venus, Mars, and the Earth. Recent technological developments make these magnetosheaths valuable potential targets for high-cadence wide-field-of-view soft X-ray imagers.Section 2 describes proposed dayside interaction mechanisms, including reconnection, the Kelvin-Helmholtz instability, and other processes in greater detail with an emphasis on the plasma density structures that they generate. It focuses upon the questions that remain as yet unanswered, such as the significance of each proposed interaction mode, which can be determined from its occurrence pattern as a function of location and solar wind conditions. Section 3 outlines the physics underlying the charge exchange generation of soft X-rays. Section 4 lists the background sources (helium focusing cone, planetary, and cosmic) of soft X-rays from which the charge exchange emissions generated by solar wind exchange must be distinguished. With the help of simulations employing state-of-the-art magnetohydrodynamic models for the solar wind-magnetosphere interaction, models for Earth’s exosphere, and knowledge concerning these background emissions, Sect. 5 demonstrates that boundaries and regions such as the bow shock, magnetosheath, magnetopause, and cusps can readily be identified in images of charge exchange emissions. Section 6 reviews observations by (generally narrow) field of view (FOV) astrophysical telescopes that confirm the presence of these emissions at the intensities predicted by the simulations. Section 7 describes the design of a notional wide FOV “lobster-eye” telescope capable of imaging the global interactions and shows how it might be used to extract information concerning the global interaction of the solar wind with solar system obstacles. The conclusion outlines prospects for missions employing such wide FOV imagers.     

叶轮行波振动下的气动阻尼计算

为展开运动边界下离心叶轮流场的数值分析,独立开发了网格变形程序和非定常流动模拟程序,实现了流场中振动离心叶轮的气动阻尼计算。采用紧支径向基函数法进行结构到气动表面变形的数据传递,应用二叉树技术进行壁面距离的计算,大幅提高了网格变形和流场分析中距离搜索的计算效率。通过振动叶栅和径向叶轮的算例,验证了程序应用于运动边界流场计算和叶轮流场模拟的正确性。以半开式叶轮为对象,展开其在行波振动条件下气动阻尼的计算分析。结果表明,叶轮在前、后行波振动下的气动阻尼均为正,后行波振动引起的气动推力和气动阻尼较大,叶轮表面的平均气动功率密度呈现循环对称的分布特征。     

航空发动机两级反向旋流燃烧室燃烧流场大涡模拟研究

为深入了解真实航空发动机内燃烧流场,采用动态亚网格模型结合单步快速化学反应(FC)、火焰面(FLM)及反应进度变量(FPV)等三种燃烧模型对径向两级反向旋流燃烧室单头部构型进行了大涡模拟。为避免模型简化误差,对燃烧室包括全部气膜冷却孔在内的精细结构进行了完全仿真。在已达到统计定常状态的冷态流场基础上首先模拟了燃料喷注和掺混过程,约2.6ms后燃料到达真实的点火位置,随后采用FPV模型在半径3mm的球形区域数值模拟了点火,展示了在主燃孔横向射流作用下初始火焰沿化学恰当比混合分数等值线传播并充满整个火焰筒的发展过程,结果显示火焰到达燃烧室出口的耗时约为6～7ms。不同模型算法预测的平均温度场与CARS测量结果作了对比,LES-FPV,RANS-FPV,LES-FLM以及参考文献中RANS-FLM计算平均误差分别为3.47%,4.17%,7.76%和11.22%,表明LES改进了模拟精度,且FPV模型显著优于FLM模型。RANS-FPV预测的出口存在严重热斑,导致其给出的出口温度分布因子(OTDF)及最大径向温度分布因子(RTDF)值分别达到0.593和0.313;LES-FPV结果均匀性最好,其预测值分别为0.284和0.193。     

Intrinsic time scale for reconnection on the dayside magnetopause

Recently much attention has been focused on the transient behavior of the magnetopause in response to pressure pulses and southward fluctuations of the interplanetary magnetic field. We examine the motion of the magnetopause behind the foreshock and conclude that this motion is affected by foreshock pressure variations but not by fluctuations in the direction of the magnetic field. Neither magnetopause erosion nor flux transfer event occurrence is controlled by the foreshock. On the contrary, flux transfer events occur at times of steady IMF and thier quasi-periodic behavior is controlled by the magnetopause or the magnetosphere and is not driven by the external boundary conditions. Since flux transfer events are clearly due to reconnection, this observation implies that the IMF must be southward some time perhaps as long as 7 minutes before flux transfer begins.     

Balloon altitude studies of southern hemisphere hard X-ray sources by the Imperial College-University of Tasmania-INPE collaboration

Hard X-ray balloon altitude measurements with a 1600 cm² phoswich array are described. Data from observations on Sco X-1, GX1+4, GX5−1, Nova Oph. 1977, SMC X-1, SS433, IC 4329A and MR 2251-178 are presented. The role of Comptonisation in X-ray production for Sco X-1 and GX1+4 is discussed.